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Close pairs: keys to comprehension of star cluster evolution

Published online by Cambridge University Press:  18 January 2010

Dany Vanbeveren
Dany Vanbeveren*
Affiliation:
Astrophysical Institute, Vrije Universiteit Brussel, Belgium email: dvbevere@vub.ac.be GroepT Leuven Engineering College, Association KU Leuven, Belgium email: dany.vanbeveren@groept.be
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Abstract

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In this review I first summarize why binaries are key objects in the study of stellar populations, to understand the evolution of star clusters and galaxies, and thus to understand the universe. I then focus on four specific topics:

  1. (i) the formation (through binaries) and evolution of very massive stars in dense clusters and the importance of stellar-wind mass loss. I discuss preliminary computations of wind mass-loss rates of very massive stars performed with the Munich hydrodynamical code and the influence of these new rates on the possible formation of an intermediate-mass black hole in the cluster MGG 11 in M82;

  2. (ii) the evolution of intermediate-mass binaries in a starburst with special emphasis on the variation of the supernova (SN) Ia rate (i.e., on the delayed time distribution of SNe Ia). A comparison with SN Ia rates in elliptical galaxies may provide important clues to SN Ia models as well as to the evolution of SN Ia progenitors;

  3. (iii) the evolution of double-neutron-star mergers in a starburst (i.e., the delayed time distribution of these mergers) and what this tells us about the suggestion that these mergers may be important production sites of r-process elements;

  4. (iv) the possible effect of massive binaries on the self-enrichment of globular clusters.

Keywords

stellar dynamicsbinaries: closestars: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S266: Star clusters: basic galactic building blocks throughout time and space , August 2009 , pp. 293 - 303
Copyright
Copyright © International Astronomical Union 2010

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